An Outer Giant Planet or Brown Dwarf in the 51 Pegasi System?

Abstract 51 Pegasi harbors the first confirmed extrasolar planet orbiting a Sun-like star. Decades of continued radial velocity (RV) observations have since uncovered signatures of an additional distant companion in the system from a shallow radial acceleration. We present new constraints on the mass and separation of a potential outer companion based on a synthesis of RVs, absolute astrometry, and new high-contrast imaging. Our analysis combines 31 yr of new and previously published RV measurements from the OHP/ELODIE, Lick/Hamilton, Keck/HIRES, and Automated Planet Finder (APF)/Levy spectrographs; a ∼25 yr baseline of absolute astrometry from Hipparcos and Gaia; and deep imaging from Keck/NIRC2 and HST/WFPC2. We find evidence for curvature in the RVs, which, when combined with nondetections from imaging and astrometry, point to a super-Jupiter at ≃15–100 au or a brown dwarf companion at ≈20–170 au. However, the inferred radial acceleration of the host star is driven primarily by the Lick/Hamilton dataset, and its slope is consistent with long-term instrument drift, calling into question the nature of the long-period signal. If an outer companion is present, it could explain the origin of the inner hot Jupiter if 51 Peg b arrived at its current location through high-eccentricity migration. On the other hand, if the signal is spurious, the exceptional baseline rules out Jovian planets within ∼10 au and most brown dwarfs within several tens of astronomical units, implying that the system is devoid of massive companions. Continued RV and astrometric monitoring together with high-contrast imaging can be used to distinguish these scenarios.